As has been shown by [1]}, the Hei 5875 Å line can be decomposed into a narrow component (NC) and a broad component (BC). The NC is generally slightly red-shifted and is believed to originate in the post-shock region near the stellar surface. The BC has been theorised to have multiple origins, with contributions from the accretion columns as well as from a hot wind. We have decomposed the Hei 5875 Å and Hei 6678 Å lines into two components in our data. Though the components vary from night to night, both profiles indeed show a clear NC and BC every night (Fig. REF ). The flux of each component varies with a similar trend, indicating that the processes that give rise to both components correlate well with each other, and therefore with accretion.
